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Exoplanet atmosphere detected

A Texas astronomer has made the first ground-based detection of an extra-solar planet's atmosphere.Provided by McDonald Observatory, Austin, Texas

Published: Thursday, December 6, 2007

The Hobby-Eberly Telescope, pictured above, made the first ground-based detection of the atmosphere of a planet outside our solar system.

Marty Harris/McDonald Observatory

December 6, 2007University of Texas at Austin astronomer and Hubble Fellow Seth Redfield has used the Hobby-Eberly Telescope (HET) at McDonald Observatory to make the first ground-based detection of the atmosphere of a planet outside our solar system.

The work is an incremental step in finding life in the universe, falling between the initial detections of planets around other stars (known as "extra-solar planets" or "exoplanets"), and the anticipated discovery of planets similar to Earth.

"What we all want to find is a planet with an Earth-like atmosphere," Redfield says.

The planet Redfield studied orbits HD189733, a star about 63 light-years away in the constellation Vulpecula, the little fox. But it's not like Earth. The planet is 20 percent more massive than Jupiter, and orbits very close to its parent star (more than 10 times closer than Mercury is to our Sun).

From Earth's line of sight, the planet passes directly in front of the star on each orbit. It was this 'transit' property that allowed the planet's discovery in 2004 by Francois Bouchy of France's Laboratoire d'Astrophysique de Marseille, and the detection of its atmosphere in 2007 by Redfield.

HD189733b is a “hot Jupiter”-type extrasolar planet. It is 20% more massive than Jupiter, but orbits 10 times closer to its star than Mercury orbits the Sun. Mercury’s orbit around the Sun is shown for comparison.

S. Redfield/T. Jones/McDonald Obs

That means this planet, HD189733b, is what's known as a "transiting extra-solar planet."

Astronomers have only once before detected the atmosphere of a planet orbiting another star in such a way, using a now inoperable instrument on Hubble Space Telescope, the Space Telescope Imaging Spectrograph (STIS).

"STIS broke soon after the detection, and there was no capability to do this from space. Ground-based observations are the only option at this time," Redfield says.

The feat has been tried unsuccessfully several times from the ground in recent years, he says. In most cases, astronomers had studied their target stars through only one transit.

"I knew we had to take it one step further," Redfield says. "I knew that we would probably have to go for many transits" to detect the atmosphere. He studied 11 transits over the course of a year with HET and its High Resolution Spectrograph.

To obtain the planet's "transmission spectrum," and thus the chemical composition of its atmosphere, he used what he called "a very straightforward" technique.

"Take a spectrum of the star when the planet is in front of the star," he says. "Then take a spectrum of the star when it's not. Then you divide the two and get the planet's atmospheric transmission spectrum."

Straightforward, but not easy. The light blocked by the planet is a mere 2.5 percent of the star's total light, plus another 0.3 percent for the planet's atmosphere.

"Each time the planet passes in front of the star," Redfield says, "the planet blocks some of the star's light. If the planet has no atmosphere, it will block the same amount of light at all wavelengths. However, if the planet has an atmosphere, gasses in its atmosphere will absorb some additional light."

Redfield used HET’s High Resolution Spectrograph to detect the well-known signature of sodium, a pair of absorption lines known as a “doublet,” at specific wavelengths (indicated here in angstroms) in the atmosphere of the extra-solar planet HD189733b.

S. Redfield/T. Jones/McDonald Obs

It was predicted that sodium atoms should be present in the atmosphere. The atmosphere of the planet will absorb more starlight at those wavelengths that correspond to specifictransitions of the sodium atom.

"This causes the planet to appear larger, since we now 'see' the planet plus the atmosphere, and we measure more blocked light from the star," Redfield says.

When studying the planet at the particular wavelength of the sodium transition, the planet appears about 6 percent larger than at other wavelengths. The detection of sodium waspossible because there's a lot of it there, and the atomic transition is strong and falls within the visual range that ground-based telescopes can detect.

"Many other atomic and molecular constituents of the atmosphere may be studied in a similar way, including potassium and hydrogen," Redfield says.

"I look forward to the detection of other gasses around this planet," Lambert says. And, "I wish every success for Seth as he chases oxygen, water vapor and other molecules --indicators of life,around planets far more accommodating to life than this one."

The dotted line shows the planet's orbit around the star HD189733. The planet orbits the star once every 2.2 Earth days, crossing the face of the star well below its equator. The small circles indicate the planet’s location during each of Seth Redfield’s more than 200 HET observations over the course of one Earth year. The red circles indicate observations during transit; the rest of the circles denote out-of-transit observations.

S. Redfield/T. Jones/McDonald Obs

The data analysis involved studying hundreds of observations spread over a year, taken under different conditions. Redfield and his collaborators removed contamination to the data caused by water vapor in Earth's own atmosphere, modeled how the star itself may have contributed to their measurements, and more, to make sure their detection was sound.

In the end, the extra-solar planet's "transmission spectrum" from HET was much higher resolution than that previously made with Hubble Space Telescope on a different planet.

"I was actually surprised and encouraged that it was even possible," Redfield says. "We've proved that it's possible. Let's start doing this for other transiting planets. Let's start doing 'comparative exoplanetology'."

"It is just breathtaking how fast the progress in the field of exoplanets is," says Redfield's collaborator, Michael Endl. "We have arrived at a point where we can study the composition of the atmospheres of 'hot Jupiters' in great detail. The HET is not only a planet finder now, but also a great tool to examine the atmospheric features of transiting extrasolar planets with unprecedented resolution. I can't wait to see how the results for the other planets will compare to our initial findings."